factors affecting use of ccds for precision astronomy
DESCRIPTION
Factors Affecting use of CCDs for Precision Astronomy. Andrew Holland , Neil Murray, Konstantin Stefanov. Talk Summary. Missions we are working on : Gaia (2013) (precision Astrometry) Euclid (2020) (weak lensing though accurate PSF shape measurement) - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/1.jpg)
Factors Affecting use of CCDs for Precision Astronomy
Andrew Holland, Neil Murray, Konstantin Stefanov
1
![Page 2: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/2.jpg)
2
Talk Summary
• Missions we are working on :– Gaia (2013) (precision Astrometry)– Euclid (2020) (weak lensing though accurate PSF shape measurement)– JUICE, LSST, Plato, Solar-C, Sentinel-4,…
• Understanding radiation damage effects on PSF shape• Trap identification techniques; CTE, EPER, Pocket Pumping• Blooming in CCDs• Clocked anti-blooming• Large signal re-distribution leading to non-linear PTCs and PSF shape distortion
Euclid PlatoGaia
![Page 3: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/3.jpg)
3
Just focussing on the Euclid Mission…
Euclid - VIS Weak Lensing PSF Requirement CCD273
Measurement is affected by - Radiation Damage to CTI (~300x spec.)- Signal re-distribution
![Page 4: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/4.jpg)
4
What We Are Doing
Radiation DamageStudies
CTI MeasurementsX-ray, EPER, PP
Thin Oxide EffectsBlooming etc
Hardening design and operation
Clocked Anti-Blooming
Clock-Induced Charge (CIC)
PP+CIC forCalibration
Mitigation & Correction
ModellingActivities
Silvaco in 3Dand 2D
Monte CarloModelling
Trapping/De-Trapping
PSF Shape Models
Corrective Modelling
Charge Re-Distribution
PTC non-linearity
PSF Distortions~10 people working on aspects of simulation, measurement and mission activities
Neil Murray Jason Gow
Edgar AllanwoodBen Dryer
David HallKonstantin Stefanov
Andy ClarkeDavid Burt
![Page 5: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/5.jpg)
5
Generation of Accurate 3D Models of the CCDs
• Extensive 3D modelling of the Euclid CCD271 to give signal volume versus size
100
101
102
103
104
105
100
101
102
Signal Size (Electrons)
Cha
rge
Pac
ket V
olum
e ( m
-3)
204 Register273 RegisterPixel
![Page 6: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/6.jpg)
6
Tri-level parallel clocking sequence
1st implementation
![Page 7: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/7.jpg)
7
Multi-level well models – Silvaco (KS)
Tri-level Quad-level
Traps causing CTI with 2 level clocking
Traps causing CTI with 3 level clocking – smaller volume of Si
![Page 8: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/8.jpg)
8
Results with Tri-level clocking
Neil Murray , 8th May 2013
![Page 9: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/9.jpg)
9
Pocket Pumping – Sub-pixel trap locations
From sequence diagrams collecting phase traps are not pumped.
Phase 1 trap – trap is in bright pixel
Readout direction
Phase 4 trap – trap is in dark pixel
![Page 10: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/10.jpg)
10
Trap pumping efficiency vs. temp
Changing the device temperature will change the emission time constants of the traps.
Trap pumping efficiency vs. temp
![Page 11: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/11.jpg)
11
Gain calibration
A number intrinsic traps are present in any CCD. Pre-flight these can be calibrated in terms of pumping efficiency under the strict operating conditions for the mission (transfer time and temperature) to a known signal such as Fe55.
This then allows the pumped signal for the same number of cycles and similar background level to be converted into electrons.
Only at the point that additional radiation induced traps interfere with a known trap does its gain calibration become unreliable. However as there are many to use the probability of losing gain calibration for each device remains low.
Histogram of a multiple serial register trap samples pumped at 70 kHz and 200 kHz
![Page 12: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/12.jpg)
12
Trap identification through te determinationCCD204 (12 µm square pixel) at -114 °C (159K) measured by CEI using 55Fe
Proton-irradiated (10 MeV) results show te ~ 1.5 secondsn.b. this data set took about 1 week to generate
Traps/pixel
0.2
0.1
![Page 13: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/13.jpg)
13
Effective te values (loss ~ 63% of maximum) shown by:
Example of te determination – parallel (slow A)CCD273 (12 µm square pixel) measured by CEI using edge response
![Page 14: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/14.jpg)
14
Plotted results are from the following work:• Black - CEI from EUCLID testing (CCD204 & CCD273)• Green - SIRA from Gaia testing (CCD91)• Red - JPL from WFC3 HST testing (CCD44). :
Divacancy (V-V--)
E-centre (P-V)
Divacancy (V-V-)
A-centre
?
Trap Release Time Measurements(note these data points are created from staff months of effort!!)
![Page 15: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/15.jpg)
15
Compilation of all known proton-irradiated te values in e2v n-channel CCDs
Trap ET eV σ x 10-15 cm² Possible type Density
A 0.46 4 E-centre (P-V) 2 x 1010 /cm³
B 0.39 7 Divacancy (V-V-) 1 x 1010 /cm³
C 0.30 5 ? None
D 0.21 0.5 Divacancy (V-V--) 1 x 109 /cm³
E 0.17 10 A-centre (O-V) 1 x 1010 /cm³
The densities are after an irradiation of ~ 1 x 109 protons/cm² (10 MeV).
• These trap species are then used in modelling used to correct for the PSF distortions in missions such as Euclid
![Page 16: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/16.jpg)
16
So we are getting on-top of traps in the CCD…..
• Unless we move to p-channel CCDs!• In which case we start over again…
• Early results were generated using setting optimisedfor n-channel CCDs
• However, indicates that devices could be up to 10x harder• A major characterisation study is now underway for ESA
Fe55 events, 1,000 transfersT=153K
1E11p.cm-2 (10 MeV equivalent)
X-ray Row Stack Plots reduce in gradient with increased toitoi = 14 µs
toi =1,000 µs
![Page 17: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/17.jpg)
17
Blooming in Thin Gate CCDs
• The field structure close to the gate oxide is different in the thin-oxide CCDs developed for enhanced space radiation tolerance
• Thin gate dielectrics are being used on SDO, Euclid and Plato• The blooming profile of the PSFs can change depending on gate bias• Vertical blooming switches to horizontal blooming
![Page 18: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/18.jpg)
18
Two-level clocking/CAB• Using potential well model• Charge is collected under phases 2 and 3• As the well capacity is exceeded (green), charge
comes into contact with the surface (red)• Surface traps (o) begin to fill with excess charge• 10’s of thousands of surface traps per pixel
• Before all the surface traps are filled, the pixel is clocked forward by 1 electrode
• Phase 2 is now pinned by taking it negative and the trapped charge is annihilated
• Surface traps under phase 4 begin to fill with excess charge
• The pixel is clock backwards by 1 electrode to the original position
• Phase 4 is now pinned by taking it negative and the trapped charge is annihilated
• Surface traps under phase 2 begin to fill with excess charge
![Page 19: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/19.jpg)
19
Clocked Anti Blooming (CAB)• Problems associated with such a technique is Clock Induced Charge (CIC) from the high field created
by V+ and V- and Trap Pumping due to the dithering.
• Astronomers do not want to see a large noisy background from the CIC, nor do they want to see dipoles everywhere (well only in calibration frames maybe)!
• Good job we have four electrodes per pixel these days, so we can reduce the field strength and know how to optimise/de-optimise the pumping process – basically don’t dither too far!
Standard image CABed image with large CIC background
Example of trap pumping diploes
![Page 20: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/20.jpg)
Comparison of CIC generation
Two-level
Three-level
Quad-level
Neil Murray , 8860-20 26th August 2013
Pinning regime
![Page 21: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/21.jpg)
21
CIC Quad-level generation rates
2 e-
per Euclid VIS frame
20 e-
per Euclid VIS frame
200 e-
per Euclid VIS frame
0.2 e-
per Euclid VIS frame
Pinning regimeStronger CAB
Need to balance the degree of CAB against the amount of CIC which can be tolerated in the application
![Page 22: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/22.jpg)
22
Quad-Level Clocking/CAB
• Fourth level reduces the field strength between clock high and pinned gate• Want to operate in the surface full well regime to make use of surface traps (Image
clock high >10 V)• Want isolation gate to be fully pinned (<-5 V) allowing all mid band traps available for
anti-blooming
![Page 23: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/23.jpg)
23
Quad-level CAB example• 660 nm laser diode
example on CCD273• ~170 ke-/pixel/sec• Blooming observed without
CAB – charge drains into the central charge injection structure
• CAB at 40 µs per cycle• No blooming!• < 4 e- CIC per frame (could
be reduced, but at a cost to the anti-blooming rate)
• No pumping – no dipoles
Without CAB With CAB
![Page 24: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/24.jpg)
24
Signal-Dependent Signal Re-Distribution
Modelling Charge Sharing• Charge sharing in CCDs can be simulated using semiconductor device simulation
software (e.g. Silvaco) – simulated PSF shown• Silvaco includes drift and diffusion, and takes into account the changing potential of the
collecting wells. Those are signal-independent and signal-dependent charge sharing components.
• Experimentally single pixel PSF is not easy to measure due to vibrations, diffraction and focusing issues.
Modelling Charge Statistics• However, the drift/diffusion equations do not explain the statistics of the signal. • Non-linear, sub-Poisson variance routinely observed in thick, back-illuminated CCDs• This must be modelled using Monte Carlo techniques
![Page 25: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/25.jpg)
25
Point Spread Function – 2D simulation using Silvaco
Simulating 5 adjacent pixels using narrow light beam illumination from the back
– 2D simulation (1 µm thick in the third dimension)
– 10 µm pixels, 5 µm + 5 µm gates– 40 µm thickness– Fully depleted– Beam centred on a potential well
4 µm wide beam @ 600 nm
Simulation by Silvaco ATLAS in 2D : photogeneration
![Page 26: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/26.jpg)
26
Silvaco Modelling Outputs
Shared charge
Electon Density
![Page 27: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/27.jpg)
27
Charge Collection – Results
Full well capacity reached
“Blooming”
Charge sharing
![Page 28: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/28.jpg)
28
Non-Linear Signal Variance
• Despite the CCD being very linear the variance vs signal is clearly non-linear in flat-filed illumination– The effect gets stronger in thick, fully depleted devices;– The effect occurs in the image area and has something to do with the charge collection. – First reported by Mark Downing in 2006 (SPIE)
Signal: linear to 0.2% (up to 120ke-)
Signal variance: not linear
3500 ADU
3500 ADU
![Page 29: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/29.jpg)
29
Signal-Dependent Charge Collection
Ideal charge collection – no sharing
Pixel 2 has more electrons than the neighbours – incoming electrons have slightly higher chance of going to the neighbour pixels.
Pixel 2 has fewer electrons than the neighbours – incoming electrons have slightly higher chance of going to Pixel 2.
3
131j
jii nnFW
P Probability of electron sharing
![Page 30: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/30.jpg)
30
Monte Carlo Model – Simulated Results
• Simulated data shows sub-Poisson variance, introduced by charge sharing.
• Quadratic fit is a very good match:
3
131j
jii nnFW
P
Probability of charge sharing:
![Page 31: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/31.jpg)
31
Experimental Data – Wavelength Dependence
= 1/Gain [e-/ADU]
Quadratic function is an excellent fit to the data
Data courtesy of Andrew Clarke, The Open UniversityMeasured with BSI CCD204 (40 μm thick)
![Page 32: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/32.jpg)
32
Experimental Data – Dependence on CCD thickness
Quadratic function is an excellent fit to the data
Data courtesy of Mark Downing, ESO
![Page 33: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/33.jpg)
33
Dependencies and Implications
• The PTC is more non-linear:– At shorter wavelengths in BSI devices (longer electron path, higher chance of sharing)– In thicker CCDs (longer electron path, higher chance of sharing)– At lower electric fields (higher chance of sharing due to lower attraction to the wells)
• The quadratic formula could be a better way to derive system gain from the PTC:– All data up to full well can be used, there is no need to choose “linear-looking” part at
low signals• In the CCD204 data:
– The gain difference between a linear fit to all points and the quadratic fit is 23%.– The gain difference between linear fit to the first few points (almost linear PTC) and
the quadratic fit is 8%.• A paper has been submitted to IEEE Transactions on Electron Devices – available soon• The effect should occur as signal from a PSF is generated producing PSF-distortion
![Page 34: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/34.jpg)
34
Charge Redistribution Experiment
PSF+BackbroundPSF only
Spot, followed by a flat illumination (diffuse LED) – not to be confused with “flat fielding”.
Spot only.
Ideally…
![Page 35: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/35.jpg)
35
Charge Redistribution Experiment
PSF+BackbroundPSF only
Spot, followed by a flat illumination (diffuse LED) – not to be confused with “flat fielding”.
Spot only. This is what should be observed in the event of charge spreading
Ideally… However with charge redistribution
Frame 1 (Mean of 100)
![Page 36: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/36.jpg)
36
Quick and Easy Demo of Large Signal Redistribution :Line and Line+Flat Images• Generate a single line but illuminating a CCD, then dumping the image except 1 row, and
move the single row back into the image• Provide a second flash on the image• Analyse the results…
testline.img
Row
s
Columns50 100 150 200 250
900
950
1000
1050
1100
1150
testlinef latx100.img
Row
s
Columns50 100 150 200 250 300
900
950
1000
1050
1100
1150
![Page 37: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/37.jpg)
37
Averaged Line Profiles
• Peak with background is reduced by 1050 DN• Wings with background are increased by 500 DN• This result clearly demonstrates the charge
redistribution effect in the vicinity of filled potential wells
• This will affect PSF shape vs. signal size
![Page 38: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/38.jpg)
38
Spot Measurements
Studies are underway into PSF measurements
Below: Average images of spots projected with increasing brightness.
![Page 39: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/39.jpg)
39
Conclusions
• Understanding the subtle effects when using CCDs is far from complete• Radiation damage is still providing a wealth of new data leading to improved
understanding and better correction techniques when in-orbit• Significant advances have been made in optimisation of clocking in the presence of
radiation-induced traps; optimising clock periods and 3 and 4-level clocking• Clock induced charge (CIC) and Pocket pumping (PP) can be used to characterise traps in-
orbit and to provide calibration signals for system gain measurements• Recently, theoretical understanding of non-linear PTC in thick back-illuminated CCDs has
been achieved; with implications for using PTCs for gain calibration• Furthermore, the signal-dependent charge re-distribution can lead to distortions in PSF
shapes which also need calibration • In future, p-channel CCDs may be more commonplace with enhanced radiation
tolerance (requiring yet more characterisation and understanding…)
![Page 40: Factors Affecting use of CCDs for Precision Astronomy](https://reader036.vdocuments.site/reader036/viewer/2022062815/56816937550346895de09b96/html5/thumbnails/40.jpg)
40
1,603 trap-pump examples on CIC backgrounds
0 shifts1,603 cycles
1 shift2*801 cycles
3 shifts4*,401 cycles
7 shifts8*200 cycles
15 shifts16*100 cycles
31 shifts32*50 cycles
Noisy, but pattern fixed by pixel geometry
Pumping and parallel shifting can be used to smooth out this noisy pattern